Noise analysis of the Indian Pulsar Timing Array data release I

被引：7

作者：

Srivastava, Aman ^{[1
]}

Desai, Shantanu ^{[1
]}

Kolhe, Neel ^{[2
]}

Surnis, Mayuresh ^{[3
]}

Joshi, Bhal Chandra ^{[4
]}

Susobhanan, Abhimanyu ^{[5
]}

Chalumeau, Aurelien ^{[6
]}

Hisano, Shinnosuke ^{[7
]}

Nobleson, K. ^{[8
]}

Arumugam, Swetha ^{[9
]}

Kharbanda, Divyansh ^{[1
]}

Singha, Jaikhomba ^{[10
]}

Tarafdar, Pratik ^{[11
]}

Arumugam, P. ^{[10
]}

Bagchi, Manjari ^{[11
,12
]}

Bathula, Adarsh ^{[13
]}

Dandapat, Subhajit ^{[14
]}

Dey, Lankeswar ^{[15
,16
]}

Dwivedi, Churchil ^{[17
]}

Girgaonkar, Raghav ^{[18
]}

Gopakumar, A. ^{[14
]}

Gupta, Yashwant ^{[4
]}

Kikunaga, Tomonosuke ^{[7
]}

Krishnakumar, M. A. ^{[19
,20
]}

Liu, Kuo ^{[19
]}

Maan, Yogesh ^{[4
]}

Manoharan, P. K. ^{[21
]}

Paladi, Avinash Kumar ^{[22
]}

Rana, Prerna ^{[14
]}

Shaifullah, Golam M. ^{[6
,23
,24
]}

Takahashi, Keitaro ^{[25
,26
]}

机构：

[1] IIT Hyderabad, Dept Phys, Kandi 502284, Telangana, India

[2] St Xaviers Coll Autonomous, Dept Phys, Mumbai 400001, Maharashtra, India

[3] IISER Bhopal, Dept Chem, Bhopal Bypass Rd, Bhopal 462066, Madhya Pradesh, India

[4] Natl Ctr Radio Astrophys, Pune Univ Campus, Pune 411007, India

[5] Univ Wisconsin Milwaukee, Ctr Gravitat Cosmol & Astrophys, Milwaukee, WI 53211 USA

[6] Univ Milano Bicocca, Dipartimento Fis G Occhialini, Piazza Sci 3, I-20126 Milan, Italy

[7] Kumamoto Univ, Grad Sch Sci & Technol, Kumamoto 8608555, Japan

[8] BITS Pilani, Dept Phys, Hyderabad Campus, Hyderabad 500078, Telangana, India

[9] IIT Hyderabad, Dept Elect Engn, Kandi 502285, India

[10] Indian Inst Technol Roorkee, Dept Phys, Roorkee 247667, India

[11] Inst Math Sci, CIT Campus, Chennai 600113, India

[12] Homi Bhabha Natl Inst, Training Sch Complex, Mumbai 400094, India

[13] Indian Inst Sci Educ & Res, Dept Phys Sci, Mohali 140306, Punjab, India

[14] Tata Inst Fundamental Res, Dept Astron & Astrophys, Homi Bhabha Rd, Mumbai 400005, India

[15] West Virginia Univ, Dept Phys & Astron, POB 6315, Morgantown, WV 26505 USA

[16] West Virginia Univ, Ctr Gravitat Waves & Cosmol, Chestnut Ridge Res Bldg, Morgantown, WV 26505 USA

[17] Indian Inst Space Sci & Technol, Dept Earth & Space Sci, Thiruvananthapuram, Kerala, India

[18] Univ Texas Rio Grande Valley, Dept Phys & Astron, One West Univ Blvd, Brownsville, TX 78520 USA

[19] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany

[20] Univ Bielefeld, Fak Phys, Postfach 100131, D-33501 Bielefeld, Germany

[21] Univ Cent Florida, Arecibo Observ, Res Pkwy, Orlando, FL USA

[22] Indian Inst Sci, Joint Astron Programme, Bengaluru 560012, Karnataka, India

[23] INFN, Sez Milano Bicocca, Piazza Sci 3, I-20126 Milan, Italy

[24] INAF, Osservatorio Astron Cagliari, Via Sci 5, I-09047 Selargius, Italy

[25] Kumamoto Univ, Fac Adv Sci & Technol, Div Nat Sci, 2-39-1 Kurokami, Kumamoto 8608555, Japan

[26] Kumamoto Univ, Int Res Org Adv Sci & Technol, 2-39-1 Kurokami, Kumamoto 8608555, Japan

来源：

PHYSICAL REVIEW D | 2023年 / 108卷 / 02期

关键词：

GRAVITATIONAL-RADIATION; SPIN NOISE; PRECISION; SEARCH; DISPERSION; GMRT;

D O I：

10.1103/PhysRevD.108.023008

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Indian Pulsar Timing Array (InPTA) collaboration has recently made its first official data release (DR1) for a sample of 14 pulsars using 3.5 years of uGMRT observations. We present the results of single pulsar noise analysis for each of these 14 pulsars using the InPTA DR1. For this purpose, we consider white noise, achromatic red noise, dispersion measure (DM) variations, and scattering variations in our analysis. We apply Bayesian model selection to obtain the preferred noise models among these for each pulsar. For PSR J1600 - 3053, we find no evidence of DM and scattering variations, while for PSR J1909 - 3744, we find no significant scattering variations. Properties vary dramatically among pulsars. For example, we find a strong chromatic noise with chromatic index-2.9 for PSR J1939 thorn 2134, indicating the possibility of a scattering index that does not agree with that expected for a Kolmogorov scattering medium consistent with similar results for millisecond pulsars in past studies. Despite the relatively short time baseline, the noise models broadly agree with the other PTAs and provide, at the same time, well-constrained DM and scattering variations.

引用

页数：29

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